Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion

By William Bottke, D. Durda, D. Nesvorný, Robert Jedicke, A. Morbidelli, David Vokrouhlický, Harold Levison. 2005

458 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/c16965dbfc1509374ab2f7e46ba3468646a39c8f

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Citations in the corpus

Identification and Dynamical Properties of Asteroid Families (2015, unknown): “…of formation ages of the asteroid families can be used to constrain how the population of the asteroid belt collisionally evolved over time ( .g., Bottke et al., 2005a,b; Cibulková et al., 2014), and how asteroid surfaces age by space weathering (chapter by Brunetto et al. in this volume).”
The Size Distributions of Asteroid Families in the SDSS Moving Object Catalog 4 (2008, unknown): “This finding will have an influence on conclusions derived from modeling the size distribution under this assumption (e.g. Bottke et al. 2005, and references therein).”
The primordial excitation and clearing of the asteroid belt—Revisited (2006, methodology): “Reconciling the long collisional pseudo-time implied by our simulations with the much shorter estimates of Bottke et al. (2005a) will likely require a re-evaluation of both the collisional modeling of Bottke et al. (2005a) and the dynamical simulations presented here.”
Full numerical simulations of catastrophic small body collisions (2008, background): “Recent work on the asteroid belt has illustrated how combined dynamical-collisional studies may be used to infer the complex evolution of the inner solar system (Bottke et al. 2005a,b).”
The OSIRIS‐REx target asteroid (101955) Bennu: Constraints on its physical, geological, and dynamical nature from astronomical observations (2015, background): “These types of objects are thought to form by the reaccumulation of smaller components escaping from the parent asteroid with similar trajectories, leading to a gravitational aggregate (Michel et al. 2001; Bottke et al. 2005).”
Yarkovsky/YORP chronology of asteroid families (2006, background): “The change in slope is an artifact of comminution (Bottke et al., 2005b) and observational bias; it is found in all the families discussed in this paper.”
Asteroid Catalog Using AKARI: AKARI/IRC Mid-Infrared Asteroid Survey (2011, background): “The total mass and the size distribution of asteroids are crucial to understanding the history of the solar system (Bottke et al. 2005).”
A NEW CHRONOLOGY FOR THE MOON AND MERCURY (2008, methodology): “16 of Bottke et al. 2005b).”
The Complete Census of 70 μm-Bright Debris Disks within “The Formation and Evolution of Planetary Systems” Spitzer Legacy Survey of Sun-like Stars (2007, background): “…of our own solar system, we would not expect to see as much dust at cool temperatures (corresponding to location between the Kuiper Belt and asteroid belt) at any point, even allowing for various planetary orbital migration scenarios (e.g., Bottke et al. 2005; Levison &Morbidelli 2003).”
In search of the source of asteroid (101955) Bennu: Applications of the stochastic YORP model (2015, background): “Once formed, the parent body would have experienced early thermal evolution by the decay of radiogenic nuclides (e.g., McSween et al., 2002), while its surface would have been battered by impacts for billions of years of cratering events (e.g., Bottke et al., 2005a,b).”
MAIN BELT ASTEROIDS WITH WISE/NEOWISE. I. PRELIMINARY ALBEDOS AND DIAMETERS (2011, background): “Similarly, Bottke et al. (2005b) have investigated the sources and sinks of excited MBAs and the effect orbital evolution has the SFD of the Main Belt.”
THE YARKOVSKY AND YORP EFFECTS: Implications for Asteroid Dynamics (2006, methodology): “As an example, we show results from their analysis of the Erigone family, which was likely produced by the disruption of a D ∼ 110 km C-type asteroid in the inner main belt (a ∼ 2.37 AU) (Bottke et al. 2005a,b).”
Size-frequency distributions of fragments from SPH/N-body simulations of asteroid impacts: Comparison with observed asteroid families (2007, methodology): “According to modeling results, these steep SFDs eventually erode back to the same shape of the background main-belt SFD (Bottke et al., 2005c).”
Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion (2017, background): “The asteroid belt’s size distribution constrains the early collisional evolution of the belt (Bottke et al., 2005a).”
Thermal inertia of near-Earth asteroids and implications for the magnitude of the Yarkovsky effect (2007, background): “…ranges, since there are reasons to suspect that the surface properties of large asteroids may be different to those of smaller bodies: for example, Bottke et al. (2005) showed that asteroids with D > 100 km and most bodies with D > 50 km in size are likely to be primordial objects that have not…”